Solubility of carbon and nitrogen in a sulfur-bearing iron melt: Constraints for siderophile behavior at upper mantle conditions

2019 ◽  
Vol 104 (12) ◽  
pp. 1857-1865 ◽  
Author(s):  
Alexander G. Sokol ◽  
Alexander F. Khokhryakov ◽  
Yuri M. Borzdov ◽  
Igor N. Kupriyanov ◽  
Yuri N. Palyanov

Abstract Carbon solubility in a liquid iron alloy containing nitrogen and sulfur has been studied experimentally in a carbon-saturated Fe-C-N-S-B system at pressures of 5.5 and 7.8 GPa, temperatures of 1450 to 1800 °C, and oxygen fugacities from the IW buffer to log fO2 ΔIW-6 (ΔIW is the logarithmic difference between experimental fO2 and that imposed by the coexistence of iron and wüstite). Carbon saturation of Fe-rich melts at 5.5 and 7.8 GPa maintains crystallization of flaky graphite and diamond. Diamond containing 2100–2600 ppm N and 130–150 ppm B crystallizes in equilibrium with BN within the diamond stability field at 7.8 GPa and 1600 to 1800 °C, while graphite forms at other conditions. The solubility of carbon in the C-saturated metal melt free from nitrogen and sulfur is 6.2 wt% C at 7.8 GPa and 1600 °C and decreases markedly with increasing nitrogen. A 1450–1600 °C graphite-saturated iron melt with 6.2–8.8 wt% N can dissolve: 3.6–3.9 and 1.4–2.5 wt% C at 5.5 and 7.8 GPa, respectively. However, the melt equilibrated with boron nitride and containing 1–1.7 wt% sulfur and 500–780 ppm boron dissolves twice less nitrogen while the solubility of carbon remains relatively high (3.8–5.2 wt%). According to our estimates, nitrogen partitions between diamond and the iron melt rich in volatiles at DNDm/Met=0.013−0.024. The pressure increase in the Fe-C-N system affects iron affinity of N and C: it increases in nitrogen but decreases in carbon. The reduction of C solubility in a Fe-rich melt containing nitrogen and sulfur may have had important consequences in the case of imperfect equilibration between the core and the mantle during their separation in the early Earth history. The reduction of C solubility allowed C supersaturation of the liquid iron alloy and crystallization of graphite and diamond. The carbon phases could float in the segregated core liquid and contribute to the carbon budget of the overlying silicate magma ocean. Therefore, the process led to the formation of graphite and diamond, which were the oldest carbon phases in silicate mantle.

2014 ◽  
Vol 59 (2) ◽  
pp. 825-828 ◽  
Author(s):  
J. Lipart ◽  
J. Łabaj ◽  
M. Słowikowski ◽  
D. Jama

Abstract In the paper, tin elimination from liquid iron alloy via low-pressure evaporation has been analysed. The experiments were performed using a single-chamber VIM 20-50 vacuum induction furnace at 1923 K and the operating pressure of 0.05 to 557 Pa.


1973 ◽  
Vol 59 (1) ◽  
pp. 55-62 ◽  
Author(s):  
Kusuhiro MUKAI ◽  
Tokio KATO ◽  
Hiroshi SAKAO

2014 ◽  
Vol 52 (9) ◽  
pp. 707-725 ◽  
Author(s):  
A. A. Kadik ◽  
V. V. Koltashev ◽  
E. B. Kryukova ◽  
V. G. Plotnichenko ◽  
T. I. Tsekhonya ◽  
...  

Science ◽  
2019 ◽  
Vol 365 (6456) ◽  
pp. 903-906 ◽  
Author(s):  
Katherine Armstrong ◽  
Daniel J. Frost ◽  
Catherine A. McCammon ◽  
David C. Rubie ◽  
Tiziana Boffa Ballaran

The composition of Earth’s atmosphere depends on the redox state of the mantle, which became more oxidizing at some stage after Earth’s core started to form. Through high-pressure experiments, we found that Fe2+ in a deep magma ocean would disproportionate to Fe3+ plus metallic iron at high pressures. The separation of this metallic iron to the core raised the oxidation state of the upper mantle, changing the chemistry of degassing volatiles that formed the atmosphere to more oxidized species. Additionally, the resulting gradient in redox state of the magma ocean allowed dissolved CO2 from the atmosphere to precipitate as diamond at depth. This explains Earth’s carbon-rich interior and suggests that redox evolution during accretion was an important variable in determining the composition of the terrestrial atmosphere.


2015 ◽  
Vol 53 (10) ◽  
pp. 849-868 ◽  
Author(s):  
A. A. Kadik ◽  
V. V. Koltashev ◽  
E. B. Kryukova ◽  
V. G. Plotnichenko ◽  
T. I. Tsekhonya ◽  
...  

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